HDPWS

IMP 8 - MIT - best fit

ResourceID
spase://CNES/NumericalData/CDPP-AMDA/IMP-8/MIT/imp-mit-k0

Description
The MIT Faraday cup experiment on IMP 8 measures currents from solar wind ions, and from these measurements we calculate the velocity, density, and temperature of the solar wind. The IMP 8 data files consist of fine resolution data (approximately 1 minute resolution). IMP 8 spins with a period of approximately 2.7s. The Faraday Cup (FC) instrument scans the solar wind distribution stepping through a contiguous set of energy windows, one step per spacecraft spin. The FC instrument divides the spin into thirty-two, 11.25 degree angular sectors and integrates the measured currents over different angular sectors depending upon the Mode in which the instrument is operating. The border between two of the 11.25 degree angular sectors lies on the Sun-spacecraft line. The FC sensor collector plate is divided into two, semi-circular halves; the division line is parallel to the spacecraft spin plane which is approximately parallel to the ecliptic plane. The split collector allow determination of the bulk plasma flow relative to the spin plane; North/South angles refer to flows coming from above or below the spin plane respectively (flows from the South are designated as having a positive N/S angle). The bulk flow angle in the spin plane is determined from the measurements of current vs. rotation angle. The currents telemetered to the ground are the sums of currents for the two half-collectors ("A" and "B") and, for the TMS and AQM modes, also the current for the half-collector "B". Electrons are measured except for the eight angles near the Sun. The experiment has two memories only one of which is operating perfectly. As a result, only every other TMS spectrum is usable, and the time between spectra is usually twice that that would be expected from the spacecraft spin rate. The bad half-memory also limits the energy windows that can be used in the other modes, since they require both memories to hold the data. On occasion, the data are read out rapidly enough by the spacecraft to allow repeated use of the good half-memory, and the time resolution in the TMS is approximately 32 seconds.

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NumericalData

ResourceID
spase://CNES/NumericalData/CDPP-AMDA/IMP-8/MIT/imp-mit-k0
ResourceHeader
ResourceName
IMP 8 - MIT - best fit
AlternateName
IMP 8 Solar Wind Plasma Faraday Cup Data
ReleaseDate
2013-09-11 09:48:17Z
Description
The MIT Faraday cup experiment on IMP 8 measures currents from solar wind ions, and from these measurements we calculate the velocity, density, and temperature of the solar wind. The IMP 8 data files consist of fine resolution data (approximately 1 minute resolution). IMP 8 spins with a period of approximately 2.7s. The Faraday Cup (FC) instrument scans the solar wind distribution stepping through a contiguous set of energy windows, one step per spacecraft spin. The FC instrument divides the spin into thirty-two, 11.25 degree angular sectors and integrates the measured currents over different angular sectors depending upon the Mode in which the instrument is operating. The border between two of the 11.25 degree angular sectors lies on the Sun-spacecraft line. The FC sensor collector plate is divided into two, semi-circular halves; the division line is parallel to the spacecraft spin plane which is approximately parallel to the ecliptic plane. The split collector allow determination of the bulk plasma flow relative to the spin plane; North/South angles refer to flows coming from above or below the spin plane respectively (flows from the South are designated as having a positive N/S angle). The bulk flow angle in the spin plane is determined from the measurements of current vs. rotation angle. The currents telemetered to the ground are the sums of currents for the two half-collectors ("A" and "B") and, for the TMS and AQM modes, also the current for the half-collector "B". Electrons are measured except for the eight angles near the Sun. The experiment has two memories only one of which is operating perfectly. As a result, only every other TMS spectrum is usable, and the time between spectra is usually twice that that would be expected from the spacecraft spin rate. The bad half-memory also limits the energy windows that can be used in the other modes, since they require both memories to hold the data. On occasion, the data are read out rapidly enough by the spacecraft to allow repeated use of the good half-memory, and the time resolution in the TMS is approximately 32 seconds.
Acknowledgement
For papers and presentations using these data, please acknowledge the MIT Space Plasma Physics Group and the path through which you accessed the data.
Contacts
Role Person StartDate StopDate Note
1. PrincipalInvestigator spase://SMWG/Person/Alan.J.Lazarus
2. TeamMember spase://SMWG/Person/John.D.Richardson

InformationURL
Name
Readme file at SPDF
URL
Description
Text created by MIT IMP8 plasma team
AccessInformation
RepositoryID
Availability
Online
AccessRights
Open
AccessURL
Name
CDPP/AMDA HAPI Server
URL
Style
HAPI
ProductKey
imp-mit-k0
Description
Web Service to this product using the HAPI interface.
Format
CSV
Acknowledgement
Thank you for acknowledging the use of AMDA in publications with wording like "Data analysis was performed with the AMDA science analysis system provided by the Centre de Données de la Physique des Plasmas (CDPP) supported by CNRS, CNES, Observatoire de Paris and Université Paul Sabatier, Toulouse". See the Rules of the road at https://amda.cdpp.eu/help/policy.html . Please acknowledge the Data Providers.
AccessInformation
RepositoryID
Availability
Online
AccessRights
Open
AccessURL
Name
CDPP/AMDA Web application
URL
Description
Access to Data via CDPP/AMDA Web application.
Format
CSV
Format
VOTable
Format
CDF
Format
PNG
Acknowledgement
Thank you for acknowledging the use of AMDA in publications with wording like "Data analysis was performed with the AMDA science analysis system provided by the Centre de Données de la Physique des Plasmas (CDPP) supported by CNRS, CNES, Observatoire de Paris and Université Paul Sabatier, Toulouse". See the Rules of the road at https://amda.cdpp.eu/help/policy.html . Please acknowledge the Data Providers.
ProcessingLevel
Calibrated
ProviderName
NSSDC
InstrumentIDs
MeasurementType
ThermalPlasma
TemporalDescription
TimeSpan
StartDate
1973-10-31 20:10:27Z
StopDate
2006-07-26 17:10:35Z
Cadence
PT58S
ObservedRegion
Heliosphere.NearEarth
ObservedRegion
Earth.Magnetosheath
Parameter #1
Name
density
ParameterKey
imp_mit_nfit
Description
(Better, from fits) Proton number density
UCD
phys.density;phys.atmol.ionStage
Units
cm^-3
UnitsConversion
1e6>m^-3
RenderingHints
DisplayType
TimeSeries
ValidMin
0.0
ValidMax
100.0
FillValue
9999.0
Particle
ParticleType
Proton
ParticleType
Ion
Qualifier
Fit
Qualifier
Scalar
ParticleQuantity
NumberDensity
Parameter #2
Name
v_bulk
ParameterKey
imp_mit_vfit
Description
(Better, from fits) Ion Flow Velocity (aberration corrected)
UCD
phys.veloc;phys.atmol.ionStage
Units
km/s
UnitsConversion
1e3>m/s
CoordinateSystem
CoordinateRepresentation
Spherical
CoordinateSystemName
GSE
RenderingHints
DisplayType
TimeSeries
ValidMin
100.0
ValidMax
3000.0
FillValue
9999.0
Particle
ParticleType
Proton
ParticleType
Ion
Qualifier
Fit
Qualifier
Magnitude
ParticleQuantity
FlowVelocity
Parameter #3
Name
v_thermal
ParameterKey
imp_mit_vthfit
Description
(Better, from fits) Proton most-probable thermal speed (aberration corrected). Thermal speed is the most probable thermal speed (i.e., the square root of [2kT/m(proton)]). To convert thermal speed to temperature in eV, multiply 0.0052 by the square of the thermal speed; to convert to temperature [K], multiply the square of the thermal speed by 60.5.
UCD
phys.veloc;phys.atmol.ionStage
Units
km/s
UnitsConversion
1e3>m/s
RenderingHints
DisplayType
TimeSeries
ValidMin
1.0
ValidMax
500.0
FillValue
9999.0
Particle
ParticleType
Proton
ParticleType
Ion
Qualifier
Fit
Qualifier
Scalar
ParticleQuantity
ThermalSpeed
Parameter #4
Name
flow angle e/w
ParameterKey
imp_mit_velewfit
Description
(Best, from fits) Proton East/West flow angle (aberration corrected). Azimuth is E/W, meaning bulk flow from the East or the West side of the Sun respectively. Positive azimuth angle means flow from the West.
UCD
pos.posAng;phys.veloc;phys.atmol.ionStage
Units
deg
CoordinateSystem
CoordinateRepresentation
Spherical
CoordinateSystemName
GSE
RenderingHints
DisplayType
TimeSeries
ValidMin
-45.0
ValidMax
45.0
FillValue
9999.0
Particle
ParticleType
Proton
ParticleType
Ion
Qualifier
Fit
Qualifier
DirectionAngle.AzimuthAngle
ParticleQuantity
FlowVelocity
Parameter #5
Name
flow angle n/s
ParameterKey
imp_mit_velnsfit
Description
(Best, from fits) Proton North/South flow angle (aberration corrected). Azimuth is N/S, meaning bulk flow from the North or the South side of the Sun respectively. Positive azimuth angle means flow from the North.
UCD
pos.posAng;phys.veloc;phys.atmol.ionStage
Units
deg
CoordinateSystem
CoordinateRepresentation
Spherical
CoordinateSystemName
GSE
RenderingHints
DisplayType
TimeSeries
ValidMin
-45.0
ValidMax
45.0
FillValue
9999.0
Particle
ParticleType
Proton
ParticleType
Ion
Qualifier
Fit
Qualifier
DirectionAngle.AzimuthAngle
ParticleQuantity
FlowVelocity